Volume 573, January 2015
|Number of page(s)||16|
|Section||Planets and planetary systems|
|Published online||12 December 2014|
Signatures of massive collisions in debris discs
A self-consistent numerical model
1 LESIA-Observatoire de Paris, UPMC Univ. Paris 06, Univ. Paris-Diderot, 92195 Meudon Cedex, France
2 Univ. Grenoble Alpes, IPAG, 38000 Grenoble, France
3 CNRS, IPAG, 38000 Grenoble, France
4 Laboratoire AIM, Université Paris Diderot/CEA/CNRS, Institut Universitaire de France, 91191 Gif-sur-Yvette, France
Received: 30 May 2014
Accepted: 30 September 2014
Context. Violent stochastic collisional events have been invoked as a possible explanation for some debris discs displaying pronounced azimuthal asymmetries or having a luminosity excess exceeding that expected for systems at collisional steady-state. So far, no thorough modelling of the consequences of such stochastic events has been carried out, mainly because of the extreme numerical challenge of coupling the dynamical and collisional evolution of the released dust.
Aims. We perform the first fully self-consistent modelling of the aftermath of massive breakups in debris discs. We follow the collisional and dynamical evolution of dust released after the breakup of a Ceres-sized body at 6 AU from its central star. We investigate the duration, magnitude, and spatial structure of the signature left by such a violent event, as well as its observational detectability.
Methods. We use the recently developed LIDT-DD code, which handles the coupled collisional and dynamical evolution of debris discs. The main focus is placed on the complex interplay between destructive collisions, Keplerian dynamics, and radiation pressure forces. We use the GRaTer package to estimate the system’s luminosity at different wavelengths.
Results. The breakup of a Ceres-sized body at 6 AU creates an asymmetric dust disc that is homogenized by the coupled action of collisions and dynamics on a timescale of a few 105 years. After a transient period where it is very steep, the particle size distribution in the system relaxes to a collisional steady-state law after ~104 years. The luminosity excess in the breakup’s aftermath should be detectable by mid-IR photometry, from a 30 pc distance, over a period of ~106 years that exceeds the duration of the asymmetric phase of the disc (a few 105 years). As for the asymmetric structures, we derive synthetic images for the VLT/SPHERE and JWST/MIRI instruments, showing that they should be clearly visible and resolved from a 10 pc distance. Images at 1.6 μm (marginally), 11.4, and 15.5 μm show the inner disc structures, while 23 μm images display the outer disc asymmetries.
Key words: planetary systems / circumstellar matter / planets and satellites: formation / zodiacal dust
© ESO, 2014
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